the next-generation space solar observatory: the solar-c...
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The next-generation space solar observatory:
The SOLAR-C Mission
H. Hara National Astronomical Observatory of Japan
JAXA SOLAR-C WG 2015 Nov 4
APSPM in Seoul National University
SOLAR-C Proposals 2015
• AssumeJAXA+ESA+Europe+USACollabora4on;Targetlaunchyearin2023
• 1stJAXAStrategicMediumMission:– AO:2014Dec26(AnnouncementofOpportunity)– ProposedbySolar-CWG(2015Feb16)
• 4thESAMedium-classMission:– AO:2014Aug19– ProposedbyEPICconsor4um(2015Jan16)
• EPIC(EuropeanPar4cipa4onInSolar-C)2
BasicProblemsinHelio-Physics1.Originoflarge-scale
explosion
2.Hea4ngofchromosphereandcorona,
Solarwindaccelera4on
3.Magne4ccycle
PlannedsatellitesolarobservatoryledbyJAXASOLAR-CWG
Firstdetermines3Dmagne4cstructuresfromunprecedentedobserva4onsforelucida4ngbasicproblemsinHelio-Phys.
Keywords:-ChromosphericBmeasurements-0.1”–0.3”spa4alresolu4on-〜1shigh-cadenceobserva4ons-highresolu4onspectroscopy
SOLAR-C
(0.1”=70km)1. Tounderstandtheplasmadynamicsasasystemthatconnectsthesolarsurfacetothesolarcoronaandinterplanetaryspace
2. Toinves4gatetheelementaryprocessesthattakeplaceuniversallyincosmicplasmas,thebothofwhichalsocontributetothecomprehensionandthepredic4onofsolarac4vitythatcouldgiveimpactontheearthandthehumansociety.
Solar-C Project View
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BasicProblemsinHelio-Physics
2.Originoflarge-scaleexplosion
1.Hea4ngofchromosphereandcorona,
Solarwindaccelera4on
3.Magne4ccycle
PlannedsatelliteSolarobservatorypreparedbyJAXASOLAR-CW.G.
Firstdetermines3Dmagne4cstructuresfromunprecedentedobserva4onsforelucida4ngbasicproblemsinHelio-Phys.
Keywords:-ChromosphericBmeasurements-0.1”–0.3”spa4alresolu4on-〜1shigh-cadenceobserva4ons-highresolu4onspectroscopy
Science Objectives
(0.1”=70km)
SOLAR-C
1. Inves4gatetheforma4onmechanismsofthechromosphere,thecorona,andthesolarwind
2. Understandthephysicaloriginoflargescalesolarerup4onstoextractthealgorithmforpredic4on
3. Revealthemechanismofsolarspectralirradiancevaria4onoftheclimatechangeoftheearth
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Solar-C Approach�Observations of All from photosphere to corona seamlessly
as a system
• Resolvetheelementalstructuresofsolaratmospheresandobservetheirchangeswithnecessarycadences,
• Determinetheproper4esandevolu4onofthe3Dmagne4cfieldB,measuringphotosphericandchromosphericB,andes4ma4ngcoronalBfromtheformerinforma4on,
• Observeallthetemperatureregimesoftheatmosphereseamlesslyandsimultaneously,and
• Obtainspectroscopicinforma4onondynamicsofelementaryprocessestakingplaceinsolaratmosphere.
SOLAR-Cwill
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Solar-C Science Cases: �I: Forma4onmechanismsof
chromosphere,corona,andsolarwind
• Understandforma4onmechanismofspiculesandtheirinfluenceinthecorona.
• Verifythenanoflarehypothesis.• Verifythewavehea4ng.• Understandthemagne4cstructure
atthesourceregionsofsolarwindsandtheiraccelera4onmechanism.
• Understandtheprominenceforma4onmechanism.
SOLAR-Cwill
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CausallinkageinSolarAtmosphereObservations of All from photosphere to corona seamlessly
HinodeHiCCirtain et al. 2012
Photosphere
Chromopshere
0
L
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Solar-C Science Cases: �II: Mechanismoflarge-scalesolarerup4ons
andalgorithmforpredic4on
• MeasureenergybuildupprocessesinflaringandCMEregions.
• Iden4fythetriggermechanismofsolarflaresandCMEs.
• Clarifythemechanismsofdestabilizinganderup4ngoftheen4resystem.
• Understandtheprocessesoffastmagne4creconnec4on.
SOLAR-Cwill
Hinode
Emergenceofasmallbipole8
Magnetic ReconnectionStudyofaFundamentalPhysicalProcess
Haraetal.(2011)
Takasaoetal.(2012)
~3”
Shibataetal.(1995)
Yohkoh Hinode & SDO SOLAR-CSpectroscopy
Imaging
wHigh-resolution (0.3”) imaging & spectroscopy in chromosphere-corona
wHigher sensitivity (>×10) than Hinode in spectroscopy
wGrowth of sheet structure by high-cadence (>×5) obs.
wMHD shock structure for heating outflows
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Solar-C Science Cases: �III: Mechanismofsolarspectralirradiancevaria4on
thatcouldinfluencetheclimatechangeoftheearth
SOLAR-Cwill
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• UnderstandtheUVirradiancein4nymagne4cstructures.
• Constructamodelcapabletoreproducetotalandspectralsolarirradiancebyincorpora4ngfinescalemagne4cstructures.
Solar-C Science objectives (proposed in 2015)I. Formation mechanism of chromosphere, corona and solar wind
I-1 Spicule FootpointBtopology,shock,twistI-2 Nano-flarehea4ng Tinybrightening,non-thermalplasmaI-3 Wavehea4ng Wavemode,energyflux,dissipa4on
I-4 Solarwindaccelera4on BtopologyinCH,AlfvenwaveincoronaI-5 Prominence Bfieldstructure,masscircula4on
II. Physical origin of large-scale eruptions and algorithm for prediction
II-1 Energystorage Photo./chrom.BfieldmapsII-2 Triggermechanism Emergingflux,interac4onwithchrom.B
II-3 Mechanismofexplosion Largescaledynamics,currentsystem
II-4 Physicsoffastreconnec4on Currentsheet,plasmoid,shock
III. Mechanism of solar spectral irradiance variation
III-1 MechanismofUVemission UVemissionsatfinescaleBstructureIII-2 TSS/SSImodeling TSI/SSI,full-diskBmap
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Requirements �(not all shown)
• Spatial resolution: Photosphere (Ph.) / Chromosphere (Ch.): 0.1”, Ch. B: 0.3”, Transition Region (TR)/Corona: 0.3”
• Temporal resolution: 1.0 sec • FOV: Ph./Ch.: >40”×40” for 0.1” resol., >160”×130” for 0.2” resol. TR/Corona: >240” ×240” • Photometric sensitivity: Ph./Ch.: < 1%, TR/Corona: < 5% • Line of sight V: < 0.1 km/s for Ph./Ch., < 1 km/s for TR/Corona • Mag. Fields B: Photosphere BL< 2 G, BT< 70 G Chromosphere: BL< 10 G
• Simultaneous observations of photosphere to corona for targets • Continuity of observations: > 3hr for fine scale, < 2 weeks for AR • Mission life: > 3 yrs near solar activity maximum
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SOLAR-C Spacecraft
SUVIT:SolarUV-Visible-IRTelescopeEUVST:EUVSpectroscopicHCI:High-resolu4onCoronalImager
EUVST(EUVSpectrograph)
HCI
SUVIT/FG
SUVIT/SP
SUVIT/IUSUVIT/UBIS
SunSensor
Hinode
50cmdia.telescope
SUVIT/TA1.4mdiametertelescope
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SOLAR-C payload
Spectro-polarimeter(SP)
Filtergraph(FG)
EUVST(EUVSpectrograph)+IM(IrradianceMonitor)
HCI(HighResolu4onCoronalImager)
SUVITSolarUV-Visible-IRTelescope
UBISUltravioletBroadbandImager
1.4mdiametertelescope
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Regions to be observed by SOLAR-C
Corona
Chromosphere
Photosphere
fromphotosphere
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EUVST0.3”res.
280”x280”
HCI0.3”res.
410”x410”
SUVIT0.1”res.
184”x184”
SOLAR-C: Field of View (FOV)
SUVITUBIS FG SP
Hi-Res.
WideFOV
184”x184”184”x143”
61”x61”70”x70”
120”x120”
USP
UBI
FeI525CaII854HeI1083
MgII280CaII393CN388CH430Cont.432225,260
FeI525NaI589FeI617HI656CaII854HeI1083
1storderbandλ1:17–22nmλ2:69–85nmλ3:92–109nmλ4:112–128nm
HeII30.4FeIX17.1FeXVIII9.4
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Proposed International Task Share
- JAXA strategic medium mission - ESA Cosmic Vision II, M4 - US Heliophysics Decadal Survey
SUVIT-TA (JAXA, ESA)
EUVST (ESA) + IM (Irradiance Monitor)
SUVIT-FG (NASA)SUVIT-SP (JAXA, ESA)
HCI (NASA)
SUVIT-UBIS (ESA)
Launcher: JAXA S/C bus: JAXA, ESA
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Coordinated Observations
Credit:ESA/AOES
SolarOrbiter
Credit:NASA/JHUAPL
(Daniel K. Inouye Solar Telescope)
DKIST
SolarDynamicObservatoryoramissionoffull-diskobserva9ons
SOLAR-C18
SOLAR-C Proposals 2015
• AssumeJAXA+ESA+Europe+USACollabora4on;Targetlaunchyearin2023
• 1stJAXAStrategicMediumMission:– AO:2014Dec26(AnnouncementofOpportunity)– ProposedbySolar-CWG(2015Feb16)
• 4thESAMedium-classMission:– AO:2014Aug19– ProposedbyEPICconsor4um(2015Jan16)
• EPIC(EuropeanPar4cipa4onInSolar-C)19
Phase of JAXA Science Project
WG
PhaseA-1
PhaseA-2
PhaseB/C/D/E
PrePhaseA
Pre-Project1
Pre-Project2
Project
MDR(MissionDefini4onReview)
Time
AO(AnnouncementofOpportunity)
Reviews
Reviews
Reviews
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MDR Results• EPIC:notselectedbyESA(2015Jun5).• SOLAR-CProposaltoJAXA
– Fivemissions(threeScienceandtwoEngineeringmissions)proposedfortheJAXA1stStrategicMission
– 1stpriorityrecommenda4onamongthreeSciencemissionsunderacondi4on(=visibilityforinterna4onaltaskshare)byScienceAdvisoryCommimee.
– Noneamongfivewasselected.SamplereturnfromMarssatellitehasselectedasCandidatefor1stStrategicMission.
– didnotpassMDR(2015Sep)because• thecondi4onofinterna4onaltaskshareisnotsa4sfied.• somescience/technicalfeasibilityisnotwellverified.
– AssessmentofEvalua4onCommimee(EC):• Re-studybyWGwithcarefulconsidera4onofmissionsize
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Japanese Space Solar Observations1980 1990 2000 2010 2020 2030
Hinotori (Hard X-rays, γ-rays)
Yohkoh (SXR, HXR, γ-rays)
Hinode (Visible, EUV, soft X-rays)
SOLAR-C
Launch
SOLARMAXSOLARMAXSOLARMAX SOLARMAX SOLARMAX
SoundingRocket(sincelate1960’s)
Spacecrao
S520-5CN S520-22CN LaunchCLASP
Planning
Development
Operation
Yohkoh
Hinode
Planning
Hinotori
SOLAR-C ( UV, Visible, NIR, EUV )
I II
Toward Updated Proposal• TargetMissionSize:
– CostReduc4onwithFocusedScienceàSmallerSUVITwithbandselec4ons,simplerEUVST,low-costcoronalimager– Affordablesize:JAXA+Europe+ESAMoO+NASAMoO:– Synergywithothermission/facility(SOLO,DKIST,..)
• Promo4onofinterna4onalcollabora4on:– SetupScienceandTechnologyDefini4onTeaminNASA– SeekforESAMoO
• EffortonmovingfromWGtoPre-Project– Re-defini4onofSolar-Csciencetargets– Improvescienceandtechnicalfeasibilitybyfurtherstudies
MissionsofOpportunity
Tightlylinked
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Summary• SOLAR-C is a mission to understand the causal
linkage between solar magnetic fields and active phenomena on the Sun and in the heliosphere.
• SOLAR-C equips three major payloads to elucidate fundamental problems in Helio-physics
by high-resolution (0.1”−0.3”) imaging & spectroscopy with temporally stable chromospheric magnetometry.
• JAXA SOLAR-C WG is updating the SOLAR-C mission proposal with more focused science for a coming opportunity (2nd Strategic Mission) with US and European institutes.
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